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Keck Observations of the Young Metal-Poor Host Galaxy of the Super-Chandrasekhar-Mass Type Ia Supernova SN 2007if | | M. Childress
; G. Aldering
; C. Aragon
; P. Antilogus
; S. Bailey
; C. Baltay
; S. Bongard
; C. Buton
; A. Canto
; N. Chotard
; Y. Copin
; H. K. Fakhouri
; E. Gangler
; M. Kerschhaggl
; M. Kowalski
; E. Y. Hsiao
; S. Loken
; P. Nugent
; K. Paech
; R. Pain
; E. Pecontal
; R. Pereira
; S. Perlmutter
; D. Rabinowitz
; K. Runge
; R. Scalzo
; R. C. Thomas
; G. Smadja
; C. Tao
; B. A. Weaver
; C. Wu
; | | Date: |
11 Mar 2011 | | Abstract: | We present Keck LRIS spectroscopy and $g$-band photometry of the metal-poor,
low-luminosity host galaxy of the super-Chandrasekhar mass Type Ia supernova SN
2007if. Deep imaging of the host reveals its apparent magnitude to be
$m_g=23.15pm0.06$, which at the spectroscopically-measured redshift of
$z_{helio}=0.07450pm0.00015$ corresponds to an absolute magnitude of
$M_g=-14.45pm0.06$. Galaxy $g-r$ color constrains the mass-to-light ratio,
giving a host stellar mass estimate of $log(M_*/M_odot)=7.32pm0.17$. Balmer
absorption in the stellar continuum, along with the strength of the 4000AA
break, constrain the age of the dominant starburst in the galaxy to be
$t_mathrm{burst}=123^{+165}_{-77}$ Myr, corresponding to a main-sequence
turn-off mass of $M/M_odot=4.6^{+2.6}_{-1.4}$. Using the R$_{23}$ method of
calculating metallicity from the fluxes of strong emission lines, we determine
the host oxygen abundance to be $12+log(O/H)_mathrm{KK04}=8.01pm0.09$,
significantly lower than any previously reported spectroscopically-measured
Type Ia supernova host galaxy metallicity. Our data show that SN 2007if is very
likely to have originated from a young, metal-poor progenitor. | | Source: | arXiv, 1103.2324 | | Services: | Forum | Review | PDF | Favorites | |
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